The OTELO survey: faint end of the luminosity function of [O_(II)]3727 emitters at ‹z›=1.43

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Cedrés, Bernabé and Bongiovanni, Ángel and Cerviño, Miguel and Nadolny, Jakub and Cepa, Jordi and Diego, José A. and Pérez García, Ana María and Gallego Maestro, Jesús and Lara López, Maritza A. and Sánchez Portal, Miguel and González Serrano, J. Ignacio and Alfaro, Emilio J. and Navarro Martínez, Rocío and Pérez Martínez, Ricardo and González, J. Jesús and Padilla Torres, Carmen P. and Castañeda, Héctor O. and González Otero, Mauro (2021) The OTELO survey: faint end of the luminosity function of [O_(II)]3727 emitters at ‹z›=1.43. Astronomy & Astrophysics, 649 . ISSN 0004-6361

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Official URL: http://dx.doi.org/10.1051/0004-6361/202039880




Abstract

Aims. In this paper, we aim to study the main properties and luminosity function (LF) of the [O II]3727 emitters detected in the OTELO survey in order to characterise the star formation processes in low-mass galaxies at z ∼ 1.43 and to constrain the faint-end of the LF.
Methods. Here, we describe the selection method and analysis of the emitters obtained from narrow-band scanning techniques. In addition, we present several relevant properties of the emitters and discuss the selection biases and uncertainties in the determination of the LF and the star formation rate density (SFRD).
Results. We confirmed a total of 60 sources from a preliminary list of 332 candidates as [O II]3727 emitters. Approximately 93% of the emitters have masses in the range of 10^(8) < M*/M⊙ < 10^(9). All of our emitters are classified as late-type galaxies, with a lower value of (u − v) when compared with the rest of the emitters of the OTELO survey. We find that the cosmic variance strongly affects the normalisation (ϕ*) of the LF and explains the discrepancy of our results when compared with those obtained from surveys of much larger volumes. However, we are able to determine the faint-end slope of the LF, namely, α = −1.42 ± 0.06, by sampling the LF down to ∼1 dex lower than in previous works. We present our calculation of the SFRD of our sample and compare it to the value obtained in previous studies from the literature.


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©ESO 2021.This paper is dedicated to the memory of our affable colleague and friend Héctor Castañeda, who passed away on Nov. 19th., 2020. The Authors thank the anonymous referee for her/his feedback and constructive suggestions, which have contributed to significantly improve the manuscript. BC wishes to thank Carlota Leal Álvarez for her support during the development of this paper. JAdD thanks the Instituto de Astrofísica de Canarias (IAC) for its support through the Programa de Excelencia Severo Ochoa and the Gobierno de Canarias for the Programa de Talento Tricontinental grant. This work was supported by the Spanish Ministry of Economy and Competitiveness (MINECO) under the grants AYA2013 - 46724 - P, AYA2014 - 58861 - C3 - 1 - P, AYA2014 - 58861 - C3 - 2 - P, AYA2014 - 58861 - C3 - 3 - P, AYA2016 - 75808 - R, AYA2016 - 75931 - C2 - 1 - P, AYA2016 - 75931 - C2 - 2 - P and MDM-2017-0737 (Unidad de Excelencia María de Maeztu, CAB). This work was supported by the project Evolution of Galaxies, of reference AYA2017 - 88007 - C3 - 1 - P, within the "Programa estatal de fomento de la investigación científica y técnica de excelencia del Plan Estatal de Investigación Científica y Técnica y de Innovación (2013-2016)" of the "Agencia Estatal de Investigación del Ministerio de Ciencia, Innovación y Universidades", and co-financed by the FEDER "Fondo Europeo de Desarrollo Regional". This article is based on observations made with the Gran Telescopio Canarias (GTC) at Roque de los Muchachos Observatory of the Instituto de Astrofísica de Canarias on the island of La Palma. This study makes use of data from AEGIS, a multiwavelength sky survey conducted with the Chandra, GALEX, Hubble, Keck, CFHT, MMT, Subaru, Palomar, Spitzer, VLA, and other telescopes, and is supported in part by the NSF, NASA, and the STFC. Based on observations obtained with MegaPrime/MegaCam, a joint project of
the CFHT and CEA/IRFU, at the Canada–France–Hawaii Telescope (CFHT) which is operated by the National Research Council (NRC) of Canada, the Institut National des Science de l’Univers of the Centre National de la Recherche Scientifique (CNRS) of France, and the University of Hawaii. This work is based in part on data products produced at Terapix available at the Canadian Astronomy Data Centre as part of the Canada-France-Hawaii Telescope Legacy Survey, a collaborative project of NRC and CNRS. Based on observations obtained with WIRCam, a joint project of CFHT, Taiwan, Korea, Canada, France, at the Canada–France–Hawaii Telescope (CFHT), which is operated by the National Research Council (NRC) of Canada, the Institute National des Sciences de l’Univers of the Centre National de la Recherche Scientifique of France, and the University of Hawaii. This work is based in part on data products produced at TERAPIX, the WIRDS (WIRcam Deep Survey) consortium, and the Canadian Astronomy Data Centre. This research was supported by a grant from the Agence Nationale de la Recherche ANR-07-BLAN-0228.

Uncontrolled Keywords:Star-forming galaxies; Emission-line galaxies; H-alpha emitters; Plus O III); France redshift survey; Similar-to O.5; Stellar mass; Formation history; Cosmic variance; Size evolution
Subjects:Sciences > Physics > Astrophysics
Sciences > Physics > Astronomy
ID Code:67831
Deposited On:21 Sep 2021 09:05
Last Modified:22 Sep 2021 10:17

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